Stellar astrophysics relies on precise and accurate measurements of stellar parameters. Over the past decade, high-precision photometric space missions such as CoRoTCoRoT: Convection, Rotation et Transits planétaires, Kepler, and TESSTESS: Transiting Exoplanet Survey Satellite [1]}, [2]}, [3]} have led to significant progress in this direction. As a result of the unprecedented performance of these missions, tens of thousands of stars have been characterized through asteroseismology. Among the different types of pulsating stars [4]}, solar-like oscillators are the most observed. The vast majority of solar-like oscillators observed by Kepler are red giants (RGs) because most targets were observed at a 29.4244 min cadence, which does not allow us to detect oscillations of main-sequence (MS) and subgiant stars. In total, solar-like pulsations were detected for more than 20 000 RG and 500 MS stars [5]}, [6]}, [7]}.
